Abstract New Canadian Galactic Plane Survey radio continuum, ROSAT X-ray, and
optical line observations of supernova remnant (SNR) 3C 434.1 (G94.0+1.0) are
presented. A radio spectrum of index
(where
) confirms this SNR's emission signature as predominantly
synchrotron, and suggests the SNR is in the Sedov expansion phase. The
morphology of the remnant is compared in X-ray, optical, and radio
continuum, and the brightest emission in all three wavelength regimes is from
the eastern hemisphere of 3C 434.1, which marks where the SNR shock is
interacting with the inside wall of its stellar wind bubble (SWB) home. The
system is determined to be 4.5 kpc distant, residing in the Perseus Arm Spiral
shock. From a deep H mosaic of the region, 656 nm H
line emission is observed that correlates well with radio synchrotron emission
and anticorrelates with X-ray emission from the SNR. The origin of this
optical emission is likely dense (
cm-3) cooling
from the wall of the SWB, where the SNR shock has penetrated and become
radiative (
km s-1). The X-ray spectrum of this SNR
between 0.5 and 2.4 keV is well modelled by a single-temperature thermal
plasma (
K,
cm-3). The magnetic
field of the bright radio synchrotron emission region is found (under the
assumption of near equipartition) to be G, a factor of 3 compression of the ambient ISM field (5 G). The westward extension of
3C 434.1 is the result of ongoing free expansion of the shock into the lower
density interior of the SWB. I use multiwavelength observations to arrive at
a unique solution for an interaction model of 3C 434.1 with the SWB, from which
the age ( yr) and mass ejected in the explosion (
) are determined. I also find an initial blast-wave velocity of
1350 km s-1, typical of type 1b SNe.